Tesis879-160308.Pdf

Total Page:16

File Type:pdf, Size:1020Kb

Tesis879-160308.Pdf FACULTAD DE CIENCIAS DEPARTAMENTO Física de la Materia Condensada TESIS DOCTORAL DEVELOPMENT OF A MARS SIMULATION CHAMBER IN SUPPORT FOR THE SCIENCE ASSOCIATED TO THE RAMAN LASER SPECTROMETER (RLS) INSTRUMENT FOR ESA'S EXOMARS MISSION Presentada por ALEJANDRO CATALÁ ESPÍ para optar al grado de doctor por la Universidad de Valladolid Dirigida por: Fernando Rull Pérez ACKNOWLEDGMENTS Mi más sincero agradecimiento a todas aquellas personas que han hecho posible que esta tesis doctoral se desarrollara. En particular: A mi director de tesis el Catedrático Fernando Rull Pérez, por darme la oportunidad de realizar esta tesis en sus instalaciones y estancias en centros de renombre en el extranjero, todo ello mediante la concesión de una beca de formación FPI. A mis compañeros de la Unidad Asociada UVa-CSIC-CAB, con especial mención a Alberto Vegas y Aurelio Sanz, por su sabiduría infinita, ayuda y disponibilidad, y a Gloria Venegas por su apoyo y complementación en aquellos aspectos ajenos a mi formación y con quien ahora tengo el placer de trabajar. A la gente de INTA, de quienes he aprendido un poco de rocket science pero sobre todo ¡a generar documentación! A todos aquellos colaboradores que han hecho que las estancias en el extranjero me ayudasen a complementar mi formación como investigador en el campo de la exploración planetaria, en especial a Pablo Sobrón y a Ian Hutchinson. Y por último, pero no por ello menos importante, a mi familia por el apoyo, cariño y ánimo recibidos desde la distancia. Sin ellos nada de esto hubiese sido posible. i TABLE OF CONTENTS ACKNOWLEDGMENTS I TABLE OF CONTENTS III TABLA DE CONTENIDOS VII INDEX OF FIGURES XI INDEX OF TABLES XV CHAPTER 1 - INTRODUCTION 1 1.1. Planetary Exploration of Mars 3 1.2. Astrobiology and Life 8 1.3. The ExoMars Programme and the 2018 ExoMars Rover 13 1.4. RLS-ExoMars and Raman spectroscopy 17 CHAPTER 2 - JUSTIFICATION AND OBJECTIVES 21 CHAPTER 3 - RLS-EXOMARS SIMULATION CHAMBER 25 3.1. Introduction 27 3.2. Pressure and temperature systems 29 3.2.1. Parts 30 3.2.1.1. RLS-ExoMars Simulation Chamber body 30 3.2.1.2. Vacuum generation station 31 iii 3.2.1.3. Pressure sensor 32 3.2.1.4. Gas and valves 33 3.2.1.5. Pressure controller 34 3.2.1.6. Refrigeration unit 35 3.2.2. Pressure and temperature test 37 3.3. Sample system 40 3.3.1. Parts 41 3.3.1.1. Refillable Container (RC) 41 3.3.1.2. Flattening subsystem 44 3.3.1.3. Optical Window 46 3.3.2. Sample system test 48 CHAPTER 4 - RLS-EXOMARS SCIENCE SIMULATOR 53 4.1. Introduction 55 4.2. Background: ExoMars RLS Simulator 57 4.3. RLS-ExoMars Science Simulator 59 4.3.1. XYZ positioning system 59 4.3.2. Optical system 60 4.3.2.1. Cube-Mounted pellicle beamsplitter 61 4.3.2.2. Raman Optical Head (OH) cylindrical adapter 62 4.3.2.3. Microscope objective ring adapter 63 4.3.2.4. Visual aid system 64 4.4. Tests 65 4.4.1. Laser power output 65 4.4.2. Laser spot size 67 4.4.3. Laser irradiance 70 4.4.4. Depth of Field (DOF) 71 4.4.5. Spectral resolution 73 4.4.6. Wavelength calibration 74 4.4.7. Optical system transfer function and intensity calibration 75 CHAPTER 5 - EXPERIMENTS 77 5.1. Introduction 79 5.2. Description of the experiments 81 iv 5.2.1. Instrumentation 81 5.3. Experiment 1: Sweep in environmental conditions 82 5.3.1. Methodology 82 5.3.2. Samples 83 5.3.2.1. Alunite 84 5.3.2.2. Gypsum 87 5.3.2.3. Jarosite 90 5.3.2.4. Quartz 93 5.4. Experiment 2: Sweep in power 95 5.4.1. Methodology 95 5.4.2. Samples 96 5.4.2.1. Jarosite 97 5.4.2.2. Hematite 119 5.5. Experiment 3: Sweep in spot size 135 5.5.1. Methodology 135 5.5.2. Samples 136 5.5.2.1. Jarosite 136 5.5.2.2. Hematite 149 5.6. Conclusions of the experiments 162 CHAPTER 6 - CONCLUSIONS 167 6.1. Conclusions of this PhD thesis 169 6.2. Future work 170 ANNEX A - PC SOFTWARE 173 ANNEX B - STEPPER MOTOR CONTROLLER 179 ANNEX C - MATLAB CODE 187 APPENDIX A - PUBLICATIONS, ABSTRACTS, REFERENCES AND MERITS 205 Publications 207 Technical documentation 207 v Abstracts 208 Oral Communications 209 Merits, Honours and transversal activities 210 References 211 APPENDIX B - RESUMEN 217 vi TABLA DE CONTENIDOS AGRADECIMIENTOS I TABLE OF CONTENTS III TABLA DE CONTENIDOS VII ÍNDICE DE FIGURAS XI ÍNDICE DE TABLAS XV CAPÍTULO 1 - INTRODUCCION 1 1.1. Exploración Planetaria de Marte 3 1.2. Astrobiología y Vida 8 1.3. El Programa ExoMars y el Rover de ExoMars 2018 13 1.4. RLS-ExoMars y la espectroscopia Raman 17 CAPÍTULO 2 - JUSTIFICACIÓN Y OBJETIVOS 21 CAPÍTULO 3 - CÁMARA DE SIMULACIÓN DE RLS-EXOMARS 25 3.1. Introducción 27 3.2. Sistemas de presión y temperatura 29 3.2.1. Partes 30 3.2.1.1. Cuerpo de la Cámara de Simulación de RLS-ExoMars 30 vii 3.2.1.2. Estación de generación de vacío 31 3.2.1.3. Sensor de presión 32 3.2.1.4. Gas y válvulas 33 3.2.1.5. Controlador de presión 34 3.2.1.6. Unidad de refrigeración 35 3.2.2. Test de presión y temperatura 37 3.3. Sistema de muestra 40 3.3.1. Partes 41 3.3.1.1. Contenedor Rellenable (RC) 41 3.3.1.2. Subsistema de aplanado 44 3.3.1.3. Ventana Óptica 46 3.3.2. Test del sistema de muestra 48 CAPÍTULO 4 - SIMULADOR DE CIENCIA DE RLS-EXOMARS 53 4.1. Introducción 55 4.2. Antecedentes: ExoMars RLS Simulator 57 4.3. Simulador de Ciencia de RLS-ExoMars 59 4.3.1. Sistema de posicionamiento XYZ 59 4.3.2. Sistema óptico 60 4.3.2.1. Divisor de haz de película montado en cubo 61 4.3.2.2. Adaptador cilíndrico de Cabezal Óptico Raman (OH) 62 4.3.2.3. Anillo adaptador de objetivo de microscopio 63 4.3.2.4. Sistema de ayuda visual 64 4.4. Tests 65 4.4.1. Potencia de salida del láser 65 4.4.2. Tamaño de spot láser 67 4.4.3. Irradiancia láser 70 4.4.4. Profundidad de campo (DOF) 71 4.4.5. Resolución espectral 73 4.4.6. Calibración en longitud de onda 74 4.4.7. Función de transferencia del sistema óptico y calibración en intensidad 75 CAPÍTULO 5 - EXPERIMENTOS 77 5.1. Introducción 79 viii 5.2. Descripción de los experimentos 81 5.2.1. Instrumentación 81 5.3. Experimento 1: Barrido en condiciones ambientales 82 5.3.1. Metodología 82 5.3.2. Muestras 83 5.3.2.1. Alunita 84 5.3.2.2. Yeso 87 5.3.2.3. Jarosita 90 5.3.2.4. Cuarzo 93 5.4. Experimento 2: Barrido en potencia 95 5.4.1. Metodología 95 5.4.2. Muestras 96 5.4.2.1. Jarosita 97 5.4.2.2. Hematite 119 5.5. Experimento 3: Barrido en tamaño de spot 135 5.5.1. Metodología 135 5.5.2. Muestras 136 5.5.2.1. Jarosita 136 5.5.2.2. Hematite 149 5.6. Conclusiones de los experimentos 162 CAPÍTULO 6 - CONCLUSIONES 167 6.1. Conclusiones de esta tesis doctoral 169 6.2. Trabajo futuro 170 ANEXO A - SOFTWARE PARA PC 173 ANEXO B - CONTROLADOR DE MOTOR PASO A PASO 179 ANEXO C - CÓDIGO MATLAB 187 APÉNDICE A - PUBLICACIONES, ABSTRACTS, REFERENCIAS Y MÉRITOS 205 Publicaciones 207 ix Documentación técnica 207 Abstracts 208 Comunicaciones orales 209 Méritos, Honores y actividades transversales 210 Referencias 211 APÉNDICE B - RESUMEN 217 x INDEX OF FIGURES Figure 1.1. - Map of the planet Mars (1877-1888) by Giovanni Schiaparelli (Credit: International Planetary Cartography Database) 3 Figure 1.2. - Misinterpretation of Schiaparelli's 'channels' by Percival Lowell (Credit: The New York Times, December 9, 1906) 4 Figure 1.3. - Three science fiction books related to Mars's intelligent beings. (a) The War of The World by H.G.Wells (public domain image), (b) A Princess of Mars, the first book of the Barsoom series by Edgar Rice Burroughs (public domain image), and (c) The Martian Chronicles by Ray Bradbury (Credit: Doubleday publishing company) 4 Figure 1.4. - Images of the Mars surface by (a) Mariner 4 (Credit: NASA) and (b) Mariner 6 and 7 (Credit: NASA) 5 Figure 1.5. - Viking 2 panorama taken at its landing site (Credit: Edward A. Guinness, Washington University in St. Louis) 5 Figure 1.6. - Sojourner rover analyzing Yogi rock (Credit: IMP Team, JPL, NASA) 6 Figure 1.7. - Comanche outcrop (at the back) found by the Spirit rover on Mars. It is composed, in part, of Fe-Mg carbonates. (Credit: NASA/JPL-Caltech/Cornell University) 6 Figure 1.8. - Gale crater and the landing elipse for MSL. Gale crater is a layered mound of clays and sulphates. (Credit: NASA / JPL-Caltech / ESA / DLR / FU Berlin / MSSS) 7 Figure 1.9. - Mars global map. A clear difference in height can be observed between smooth northern highlands and the rugged southern lowlands. (Credit: MOLA Science Team) 11 Figure 1.10. - SEM image for ALH84001 interpreted biogenic microstructures (Credit: NASA) 12 Figure 1.11. - Elements of the ExoMars Programme: the Trace Gas Orbiter (TGO) on the upper left and the ExoMars Rover on the lower right.
Recommended publications
  • Infrared Experiments for Spaceborne Planetary Atmospheres Research Full Report
    NASA Technical Memorandum 84414 Infrared Experiments for Spaceborne Planetary Atmospheres Research Full Report Infrared Experiments Working Group NOVEMBER 1981 NASA NASA Technical Memorandum 84414 Infrared Experiments for Spaceborne Planetary Atmospheres Research Full Report Infrared Experiments Working Group Jet Propulsion Laboratory Pasadena, California NASA National Aeronautics and Space Administration Scientific and Technical Information Branch 1981 TABLE OF CONTENTS Preface Summary of Principal Conclusions and Recommendations Chapter I The Role of Infrared Sensing in Atmospheric Science Chapter II Review of Existing Infrared Measurement Techniques Chapter III Critical Comparison of Proposed Measurement Techniques Chapter IV Conclusions and Recommended Instrument Developments Appendices: A Critical Technologies B Applicability of Atmospheric Infrared Instrumentation to Surface Science C Supporting Studies in Data Analysis and Numerical Modeling D Description of Planned Earth Orbital Platforms ii PREFACE Experiments conducted in the infrared spectral region provide a powerful tool for the study of the composition, structure and dynamics of planetary atmospheres. However, the field has become highly complex, especially that part associated with spacecraft sensing, and the range of technologies used so diverse that it is difficult to determine which of the available methods for making a particular measurement is to be preferred, even for those deeply involved in the field. Unfortunately, the realities of the age demand that some selectivity be employed; not all approaches can be supported. Furthermore, the chosen methods are generally sufficiently untried that long pre-flight developments are neces- sary if viable proposals are to be written for future flight opportunities. These considerations clearly lead to a program of developments which must be coordinated on a national scale.
    [Show full text]
  • EDL – Lessons Learned and Recommendations
    ."#!(*"# 0 1(%"##" !)"#!(*"#* 0 1"!#"("#"#(-$" ."!##("""*#!#$*#( "" !#!#0 1%"#"! /!##"*!###"#" #"#!$#!##!("""-"!"##&!%%!%&# $!!# %"##"*!%#'##(#!"##"#!$$# /25-!&""$!)# %"##!""*&""#!$#$! !$# $##"##%#(# ! "#"-! *#"!,021 ""# !"$!+031 !" )!%+041 #!( !"!# #$!"+051 # #$! !%#-" $##"!#""#$#$! %"##"#!#(- IPPW Enabled International Collaborations in EDL – Lessons Learned and Recommendations: Ethiraj Venkatapathy1, Chief Technologist, Entry Systems and Technology Division, NASA ARC, 2 Ali Gülhan , Department Head, Supersonic and Hypersonic Technologies Department, DLR, Cologne, and Michelle Munk3, Principal Technologist, EDL, Space Technology Mission Directorate, NASA. 1 NASA Ames Research Center, Moffett Field, CA [email protected]. 2 Deutsches Zentrum für Luft- und Raumfahrt e.V. (DLR), German Aerospace Center, [email protected] 3 NASA Langley Research Center, Hampron, VA. [email protected] Abstract of the Proposed Talk: One of the goals of IPPW has been to bring about international collaboration. Establishing collaboration, especially in the area of EDL, can present numerous frustrating challenges. IPPW presents opportunities to present advances in various technology areas. It allows for opportunity for general discussion. Evaluating collaboration potential requires open dialogue as to the needs of the parties and what critical capabilities each party possesses. Understanding opportunities for collaboration as well as the rules and regulations that govern collaboration are essential. The authors of this proposed talk have explored and established collaboration in multiple areas of interest to IPPW community. The authors will present examples that illustrate the motivations for the partnership, our common goals, and the unique capabilities of each party. The first example involves earth entry of a large asteroid and break-up. NASA Ames is leading an effort for the agency to assess and estimate the threat posed by large asteroids under the Asteroid Threat Assessment Project (ATAP).
    [Show full text]
  • Mariner to Mercury, Venus and Mars
    NASA Facts National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, CA 91109 Mariner to Mercury, Venus and Mars Between 1962 and late 1973, NASA’s Jet carry a host of scientific instruments. Some of the Propulsion Laboratory designed and built 10 space- instruments, such as cameras, would need to be point- craft named Mariner to explore the inner solar system ed at the target body it was studying. Other instru- -- visiting the planets Venus, Mars and Mercury for ments were non-directional and studied phenomena the first time, and returning to Venus and Mars for such as magnetic fields and charged particles. JPL additional close observations. The final mission in the engineers proposed to make the Mariners “three-axis- series, Mariner 10, flew past Venus before going on to stabilized,” meaning that unlike other space probes encounter Mercury, after which it returned to Mercury they would not spin. for a total of three flybys. The next-to-last, Mariner Each of the Mariner projects was designed to have 9, became the first ever to orbit another planet when two spacecraft launched on separate rockets, in case it rached Mars for about a year of mapping and mea- of difficulties with the nearly untried launch vehicles. surement. Mariner 1, Mariner 3, and Mariner 8 were in fact lost The Mariners were all relatively small robotic during launch, but their backups were successful. No explorers, each launched on an Atlas rocket with Mariners were lost in later flight to their destination either an Agena or Centaur upper-stage booster, and planets or before completing their scientific missions.
    [Show full text]
  • The Pancam Instrument for the Exomars Rover
    ASTROBIOLOGY ExoMars Rover Mission Volume 17, Numbers 6 and 7, 2017 Mary Ann Liebert, Inc. DOI: 10.1089/ast.2016.1548 The PanCam Instrument for the ExoMars Rover A.J. Coates,1,2 R. Jaumann,3 A.D. Griffiths,1,2 C.E. Leff,1,2 N. Schmitz,3 J.-L. Josset,4 G. Paar,5 M. Gunn,6 E. Hauber,3 C.R. Cousins,7 R.E. Cross,6 P. Grindrod,2,8 J.C. Bridges,9 M. Balme,10 S. Gupta,11 I.A. Crawford,2,8 P. Irwin,12 R. Stabbins,1,2 D. Tirsch,3 J.L. Vago,13 T. Theodorou,1,2 M. Caballo-Perucha,5 G.R. Osinski,14 and the PanCam Team Abstract The scientific objectives of the ExoMars rover are designed to answer several key questions in the search for life on Mars. In particular, the unique subsurface drill will address some of these, such as the possible existence and stability of subsurface organics. PanCam will establish the surface geological and morphological context for the mission, working in collaboration with other context instruments. Here, we describe the PanCam scientific objectives in geology, atmospheric science, and 3-D vision. We discuss the design of PanCam, which includes a stereo pair of Wide Angle Cameras (WACs), each of which has an 11-position filter wheel and a High Resolution Camera (HRC) for high-resolution investigations of rock texture at a distance. The cameras and electronics are housed in an optical bench that provides the mechanical interface to the rover mast and a planetary protection barrier.
    [Show full text]
  • 18Th EANA Conference European Astrobiology Network Association
    18th EANA Conference European Astrobiology Network Association Abstract book 24-28 September 2018 Freie Universität Berlin, Germany Sponsors: Detectability of biosignatures in martian sedimentary systems A. H. Stevens1, A. McDonald2, and C. S. Cockell1 (1) UK Centre for Astrobiology, University of Edinburgh, UK ([email protected]) (2) Bioimaging Facility, School of Engineering, University of Edinburgh, UK Presentation: Tuesday 12:45-13:00 Session: Traces of life, biosignatures, life detection Abstract: Some of the most promising potential sampling sites for astrobiology are the numerous sedimentary areas on Mars such as those explored by MSL. As sedimentary systems have a high relative likelihood to have been habitable in the past and are known on Earth to preserve biosignatures well, the remains of martian sedimentary systems are an attractive target for exploration, for example by sample return caching rovers [1]. To learn how best to look for evidence of life in these environments, we must carefully understand their context. While recent measurements have raised the upper limit for organic carbon measured in martian sediments [2], our exploration to date shows no evidence for a terrestrial-like biosphere on Mars. We used an analogue of a martian mudstone (Y-Mars[3]) to investigate how best to look for biosignatures in martian sedimentary environments. The mudstone was inoculated with a relevant microbial community and cultured over several months under martian conditions to select for the most Mars-relevant microbes. We sequenced the microbial community over a number of transfers to try and understand what types microbes might be expected to exist in these environments and assess whether they might leave behind any specific biosignatures.
    [Show full text]
  • Raman Spectroscopy of Shocked Gypsum from a Meteorite Impact Crater
    International Journal of Astrobiology 16 (3): 286–292 (2017) doi:10.1017/S1473550416000367 © Cambridge University Press 2016 This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited. Raman spectroscopy of shocked gypsum from a meteorite impact crater Connor Brolly, John Parnell and Stephen Bowden Department of Geology & Petroleum Geology, University of Aberdeen, Meston Building, Aberdeen, UK e-mail: c.brolly@ abdn.ac.uk Abstract: Impact craters and associated hydrothermal systems are regarded as sites within which life could originate onEarth,and onMars.The Haughtonimpactcrater,one ofthemost well preservedcratersonEarth,is abundant in Ca-sulphates. Selenite, a transparent form of gypsum, has been colonized by viable cyanobacteria. Basementrocks, which havebeenshocked,aremoreabundantinendolithicorganisms,whencomparedwithun- shocked basement. We infer that selenitic and shocked gypsum are more suitable for microbial colonization and have enhanced habitability. This is analogous to many Martian craters, such as Gale Crater, which has sulphate deposits in a central layered mound, thought to be formed by post-impact hydrothermal springs. In preparation for the 2020 ExoMars mission, experiments were conducted to determine whether Raman spectroscopy can distinguish between gypsum with different degrees of habitability. Ca-sulphates were analysed using Raman spectroscopyand resultsshow nosignificant statistical difference between gypsumthat has experienced shock by meteorite impact and gypsum, which has been dissolved and re-precipitated as an evaporitic crust. Raman spectroscopy is able to distinguish between selenite and unaltered gypsum. This showsthat Raman spectroscopy can identify more habitable forms of gypsum, and demonstrates the current capabilities of Raman spectroscopy for the interpretation of gypsum habitability.
    [Show full text]
  • Complete List of Contents
    Complete List of Contents Volume 1 Cape Canaveral and the Kennedy Space Center ......213 Publisher’s Note ......................................................... vii Chandra X-Ray Observatory ....................................223 Introduction ................................................................. ix Clementine Mission to the Moon .............................229 Preface to the Third Edition ..................................... xiii Commercial Crewed vehicles ..................................235 Contributors ............................................................. xvii Compton Gamma Ray Observatory .........................240 List of Abbreviations ................................................. xxi Cooperation in Space: U.S. and Russian .................247 Complete List of Contents .................................... xxxiii Dawn Mission ..........................................................254 Deep Impact .............................................................259 Air Traffic Control Satellites ........................................1 Deep Space Network ................................................264 Amateur Radio Satellites .............................................6 Delta Launch Vehicles .............................................271 Ames Research Center ...............................................12 Dynamics Explorers .................................................279 Ansari X Prize ............................................................19 Early-Warning Satellites ..........................................284
    [Show full text]
  • Final Report Venus Exploration Targets Workshop May 19–21
    Final Report Venus Exploration Targets Workshop May 19–21, 2014, Lunar and Planetary Institute, Houston, TX Conveners: Virgil (Buck) Sharpton, Larry Esposito, Christophe Sotin Breakout Group Leads Science from the Surface Larry Esposito, Univ. Colorado Science from the Atmosphere Kevin McGouldrick, Univ. Colorado Science from Orbit Lori Glaze, GSFC Science Organizing Committee: Ben Bussey, Martha Gilmore, Lori Glaze, Robert Herrick, Stephanie Johnston, Christopher Lee, Kevin McGouldrick Vision: The intent of this “living” document is to identify scientifically important Venus targets, as the knowledge base for this planet progresses, and to develop a target database (i.e., scientific significance, priority, description, coordinates, etc.) that could serve as reference for future missions to Venus. This document will be posted in the VEXAG website (http://www.lpi.usra.edu/vexag/), and it will be revised after the completion of each Venus Exploration Targets Workshop. The point of contact for this document is the current VEXAG Chair listed at ABOUT US on the VEXAG website. Venus Exploration Targets Workshop Report 1 Contents Overview ....................................................................................................................................................... 2 1. Science on the Surface .............................................................................................................................. 3 2. Science within the Atmosphere ...............................................................................................................
    [Show full text]
  • Galileo in 1610
    Module 3 – Nautical Science Unit 4 – Astronomy Chapter 15 - The Planets Section 2 – Mars & Jupiter What You Will Learn to Do Demonstrate understanding of astronomy and how it pertains to our solar system and its related bodies: Moon, Sun, stars and planets Objectives 1. Describe the major features of Mars 2. Identify the principal characteristics of Jupiter Key Terms CPS Key Term Questions 1 - 5 Key Terms Nix Olympica - Snow of Olympus Galilean satellites - The four largest and brightest moons of Jupiter: Io, Europa, Ganymede and Callisto; discovered by Galileo in 1610 Prograde The counter-clockwise direction of motion - celestial bodies around the Sun as seen from above the north pole of the Sun; in the sky it is from west to east Key Terms Retrograde The clockwise direction of celestial motion - bodies around the Sun; in the sky it is from east to west Rotational axis - The straight line through all fixed points of a rotating rigid body around which all other points of the body move in circles Opening Question Discuss what types of exploration missions have occurred on Mars. (Use CPS “Pick a Student” for this question.) Mars Fourth from Mars the Sun and the next planet beyond Earth, Mars has aroused the greatest interest. Mars Mars Ares (Roman Mars) Mars Named for the Roman god of war, it is often called the “red planet.” Mars Mars’ red color and its rapid movement from west to east among the stars make it stand out in the sky. Mars Earth The best time to see Mars is when it is nearest to Earth in August and September, when the Earth is Sun between the Sun and Mars.
    [Show full text]
  • Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave
    PROCEEDINGS OF SPIE Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave Makenzie Lystrup Howard A. MacEwen Giovanni G. Fazio Editors 10–15 June 2018 Austin, Texas, United States Sponsored by 4D Technology (United States) • Andor Technology, Ltd. (United Kingdom) • Astronomical Consultants & Equipment, Inc. (United States) • Giant Magellan Telescope (Chile) • GPixel, Inc. (China) • Harris Corporation (United States) • Materion Corporation (United States) • Optimax Systems, Inc. (United States) • Princeton Infrared Technologies (United States) • Symétrie (France) Teledyne Technologies, Inc. (United States) • Thirty Meter Telescope (United States) •SPIE Cooperating Organizations European Space Organisation • National Radio Astronomy Observatory (United States) • Science & Technology Facilities Council (United Kingdom) • Canadian Astronomical Society (Canada) Canadian Space Association ASC (Canada) • Royal Astronomical Society (United Kingdom) Association of Universities for Research in Astronomy (United States) • American Astronomical Society (United States) • Australian Astronomical Observatory (Australia) • European Astronomical Society (Switzerland) Published by SPIE Volume 10698 Part One of Three Parts Proceedings of SPIE 0277-786X, V. 10698 SPIE is an international society advancing an interdisciplinary approach to the science and application of light. The papers in this volume were part of the technical conference cited on the cover and title page. Papers were selected and subject to review by the editors and conference program committee. Some conference presentations may not be available for publication. Additional papers and presentation recordings may be available online in the SPIE Digital Library at SPIEDigitalLibrary.org. The papers reflect the work and thoughts of the authors and are published herein as submitted. The publisher is not responsible for the validity of the information or for any outcomes resulting from reliance thereon.
    [Show full text]
  • Lunar and Planetary Information Bulletin, Issue
    Jet Propulsion Laboratory: Where Planetary Exploration Began Note from the Editors: This issue’s lead article is the seventh in a series of reports describing the history and current activities of the planetary research facilities funded by NASA and located nationwide. This issue features the Jet Propulsion Laboratory (JPL), which since before World War II has been a leading engineering research and development center, creating America’s first satellite and most of its lunar and planetary spacecraft. It is now a major NASA center, focusing on robotic space exploration. While JPL is also very active in Earth observation and space technology programs, this article focuses on JPL’s planetary efforts. — Paul Schenk and Renee Dotson LFrom the roar of pioneering Space Age rockets to the soft whir of servos on twenty-first-century robot explorers on Mars, spacecraft designed and built at NASA’s Jet Propulsion Laboratory (JPL) have blazed the trail to the planets and into the universe beyond for nearly 60 years. The United States (U.S.) first entered space with the 1958 launch of the satellite Explorer 1, built and controlled by JPL. From orbit, Explorer 1’s voyage yielded immediate scientific results — the discovery of the Van Allen radiation belts — and led to the creation of NASA. Innovative technology from JPL has taken humanity far beyond regions of space where we can actually travel ourselves. The most distant human-made objects, Voyagers 1 and 2, were built at and are operated by JPL. From JPL’s labs and clean rooms come telescopes and cameras that have extended our vision to unprecedented depths and distances, Ppeering into the hearts of galactic clouds where new stars and planets are born, and even toward the beginning of time at the edge of the universe.
    [Show full text]
  • Digital Processing of the Mariner 6 and 7 Pictures
    VOL. 76, NO. 2 JOURNAL OF GEOPHYSICAL RESEARCH JANUARY 10, 1971 Digital Processing of the Mariner 6 and 7 Pictures T. C. RINDFLEISC H, J. A. DUNNE, H. ,J. FRIEDEN, W. D. STHOMBEHa, AND R. M. RUIZ Space Sciences D-ivision, J et Propttls'ion Laboratory Pasaaena, California 91103 The Mariner Mars 1969 t.elevision camera system was a vidicon-based digital system and in­ cluded a complex on-board video encoding and recording scheme. The spacecraft video processing was designed to maximize the volume of data returned and the encoded discriminability of the low-contrast surface detail of Mars. The ground-based photometric reconstruction of the Mariner photographs, as well as the correction of inherent vidicon camera distortion effects necessary to achieve television experiment objectives, required use of a digit.al computer to process the pictllres. The digital techniques developed to reconstl"Uct the spacecraft encoder effects and to correct for camera distortions are described and examples shown of the processed results. Specific distortion corrections that are considered include the removal of structured system noises, the removal of sensor residual image, the correction of photometric sensitivity nonunifonnit,ies and nonlinearities, the correction of geometric distortions, and the correctrn of modulat,ion transfer limitations. As all physically realizable instruments in_/ and interpretations of the imagery can be based fluence the data they collect, the Mariner Mars on information as representative of the Martian 1969 television cameras left their signatures on surface as possible. the imagery they returned to earth. Analyses The succeeding sections will describe, from of the Mariner photographs must be performed the point of view of image processing, the per­ with the knowledge that Mars was observed formance characteristics of the vidicon cameras through the spacecraft cameras, and any distor- and data-encoding electronics on board the tions introduced by the camera system processes spacecraft, the over-all flow of the various potentially affect the results.
    [Show full text]